AGN, MASSIVE BLACK HOLES, ACCRETION OR ARE AGN FACTORIES OF HIGH ENERGY PARTICLES AND PHOTONS? Suzy Collin-Zahn LUTH, Observatoire de Paris Meudon Blois 2008

STRONG AND WEAK ACCRETORS THE CONTEXT STRONG AND WEAK ACCRETORS DICHOTOMY RADIO LOUD / RADIO QUIET OBJECTS AND JETS / WINDS CONCLUSION Blois 2008

STRONG AND WEAK ACCRETORS THE CONTEXT STRONG AND WEAK ACCRETORS DICHOTOMY RADIO LOUD / RADIO QUIET OBJECTS AND JETS / WINDS CONCLUSION Blois 2008

RECALL OF SOME WELL-KNOWN FACTS Active Galactic Nuclei: from quasars (L=1046-48 erg/s) to Seyfert galaxies (L=1043-46 erg/s), and Low Luminosity AGN (L=1040-43 erg/s) 2. Power derived from accretion onto a supermassive black hole 3. BH present in ALL NUCLEI of galaxy, M(BH) from L=1010 to 105 M , M(BH) ~ M(Bulge)/1000 4. « Unified Scheme » Blois 2008

radio galaxies LINERs Wind (FRI) (FRII) Narrow line region Broad line region Accretion disk Black hole radio galaxies LINERs Absorbing torus (RL or RQ) Wind Blois 2008 (FRI) (FRII)

Faranoff-Riley, 1974 MILLIONS OF LIGHT-YEARS Blois 2008

0.057 for a Schwarzschild BH, R(ISCO)=6Rg SOME FIDUCIAL VALUES gravitational radius: =1.5 1013 M8 cm ~10-5 pc Eddington luminosity = 1.3 1046 M8 erg/s bolometric luminosity where is the accretion rate rmaximum radiation efficiency of mass-energy conversion 0.057 for a Schwarzschild BH, R(ISCO)=6Rg 0.3 for a maximally rotating Kerr BH, R(ISCO)~1Rg Blois 2008

« ACCRETION DISKS » HOW TO FUEL BLACK HOLES? The angular momentum (GMR)1/2 must be transported outward! 1. At large distances (≥ 100pc) Major and minor mergers (quasars) Tidal interactions between galaxies (luminous Seyfert) Bars, bars within bars, nonaxisymmetric potentials (weak Seyfert) Dynamical friction of molecular clouds (LLAGN)… 2. At small distances (<1pc) « ACCRETION DISKS » local turbulent viscosity (MRI, possibly) or global transport of AM via an organized magnetic field? 3. At intermediate distances Blois 2008 Still unknown! Gravitational instability?

STRONG AND WEAK ACCRETORS THE CONTEXT STRONG AND WEAK ACCRETORS DICHOTOMY RADIO LOUD / RADIO QUIET OBJECTS AND JETS / WINDS CONSLUSION Blois 2008

Luminous AGN : ~ 1% of all galaxies In local Universe Luminous AGN : ~ 1% of all galaxies Low Luminosity AGN : ~ 40% of all galaxies The remainder 60%: dormant BH Blois 2008

INFLUENCE OF THE ACCRETION RATE ACCRETION DISKS: INFLUENCE OF THE ACCRETION RATE Blois 2008

A. STRONG ACCRETORS Spectral distribution of Seyfert and RQQ, no radio or gamma radiation, everything is thermal! thermal emission accretion hot corona thermal Compton dust cold accretion disk thermal Compton inverse Compton synchrotron Observations by Sanders et al. 1989 Blois 2008

I. Thin disks, H/R <<0.1, optically thick, emit the « Big Blue Bump » Seyfert II. « slim » disks, H/R ~0.1, optically thick, radiation pressure, emit the « Big Blue Bump » Quasars, Narrow Line Seyfert 1 (NLS1s) III. « Thick » disks, H/R~1, optically thick, radiation pressure, emit soft X-rays, photons cannot escape, thus  Blois 2008 Some low mass NLS1s (106-7Mo), in growing process

. CONTROVERSY ABOUT THICK DISKS Do these boulimic accretors exist? MHD simulations seems to show that if m >> 10 at large distance, strong outflows are expelled at smaller distance, and the accretion rate on the BH remains limited at the Eddington value. . Blois 2008

NO HARD X-RAYS ARE EXPECTED FROM THESE DISKS BUT proof of the presence of a hot medium emitting the hard X-rays whose emission is « reflected » by the disk MCG _6_30_15 Iron K line Intensity Fabian et al. 2006 Energy in keV Relativistic profile of FeK  the disk extends down to ~10Rg, and sometimes to ~1Rg  ISCO of a rapidly spinning BH Blois 2008

The reflection model: radiatively coupled disk + corona Corona Compton-cooled by UV photons Disk heated by gravitational release AND X-rays Same radiation coupling, but more realistic model : disk + « magnetic flares » Done, Gierlinski , 2004 Blois 2008

LLAGN, radio galaxies FRI (M87..), Galactic Center B. WEAK ACCRETORS Optically thin, geometrically thick, hot (relativistic) disks, emitting mainly radio and X-rays, Gas falls into the BH before radiating, thus  LLAGN, radio galaxies FRI (M87..), Galactic Center Blois 2008

…suppression of the inner regions of accretion disk Inflated codona, or… …suppression of the inner regions of accretion disk The « Big Blue Bump » does not exist Blois 2008

CONTROVERSY ABOUT THESE DISKS Which model for these anorexic accretors? ADAF, ADIOS, CDAF… RIAF Is there also a jet? Blois 2008

. ADAF+JET FOR A « QUIESCENT » BH: THE GALACTIC CENTER measured M~3 10-6 Mo /yr  L (for  ~0.1) should be ~ 1041 erg/s BUT measured L~ 1036 erg/s  L/LEdd ~ 3 10-9,  ~ 10-6 Synchrotron and Inverse Compton by thermal electrons flaring quiescent Synchrotron and Inverse Compton by non-thermal electrons (jet or ADAF?) bremsstrahlung Yuan, Quataert, Narayan, 2003 Blois 2008

a Sgr A* Jet? ~ 1 pc F. Baganoff et al. 2003 Blois 2008

ADAF+JET MODEL FOR A FRI GALAXY L/LEdd ~ 3 10-4 ADAF Jet Wu, Yuan, Cao, 2008 Blois 2008

BOTH STRONG AND WEAK ACCRETORS ARE RADIATIVELY INEFFICIENT CONCLUSION: BOTH STRONG AND WEAK ACCRETORS ARE RADIATIVELY INEFFICIENT DISKS MUST PRODUCE OUTFLOWS TO EVACUATE THEIR ENERGY Blois 2008

STRONG AND WEAK ACCRETORS THE CONTEXT STRONG AND WEAK ACCRETORS DICHOTOMY RADIO LOUD / RADIO QUIET OBJECTS AND JETS / WINDS CONCLUSION Blois 2008

AGN are divided in « Radio Loud » (RL) and « Radio Quiet » (RQ) RLQ BLRG FRI RQQ SEYFERTS LINERS Sikora, Stawarz, Lasota, 2007 Blois 2008

With a complete sample of quasars (SDSS) Mc Lure, Dunlop 2004 R = Lradio(5GHz) / Lopt Blois 2008 Number of RLQ are less than 10% of RQQ

RADIO LOUDNESS DEPENDS ON THE EDDINGTON FACTOR FRI BLRG RLQ LINERS SEYFERTS RQQ Log(L/Ledd) Blois 2008

RADIO LOUDNESS DEPENDS ON M(BH) FRI RLQ LINERS, SEYFERTS BLRG RQQ Blois 2008

WHY? I. HIGH LUMINOSITY AGN DIFFERENCES BETWEEN RL AND RQ objects 1. Locally RL are exclusively in elliptical galaxies, RQ in spiral galaxies 2. RLs are associated with non-thermal relativistic collimated jets, RQs seem associated with thermal non-collimated winds (detected by Broad Absorption Lines and X-ray absorbers) 3. Several more subtile properties, not understood (i.e. intense FeII lines only in RQs) WHY? Blois 2008

Jets are launched at R ≤ 1000 Rg (VLBI) JETS VERSUS WINDS OBSERVATIONS Jets are launched at R ≤ 1000 Rg (VLBI) Winds are launched at R ≥ 10000Rg Jets have relativistic bulk velocities and are made of relativistic particles Winds have velocities from few hundreds km/s to c/10 and consist of warm (105-6 K) thermal gas Blois 2008

Magnetic field is indispensable to explain extended jet acceleration: JET DRIVING MECHANISM Magnetic field is indispensable to explain extended jet acceleration: 1. Centrifugally driven flow 2. Extraction of the rotational energy of the BH: field connects the BH to the disk (Blandford-Znajek, 1977) W Jets might be linked with the spin of the BH Blois 2008

Measured by dimensionless angular momentum a = J/Jmax = cJ/GM2 BLACK HOLE SPIN Measured by dimensionless angular momentum a = J/Jmax = cJ/GM2 1. Even RQ AGN have spinning BH (FeK line) 2. Cosmological evolution of AGN requires large fraction of spinning BHs (mass-conversion efficiency must be > 0.06) 3. Power of the jet must increase with a 4. It is expected that a increases with accretion AND with merger of two BHs 5. BHs increase with galaxy bulges, and a fraction of elliptical galaxies (large bulges) are due to the merger of spirals Elliptical galaxies favor high spin, therefore jets Blois 2008

But it does not explain all: Other mechanisms must be at work Environnement can play a role:spiral galaxies contain cold gas, ellipticals contain and are surrounded by hot gas 2. Geometry of the inner disk can play a role: thick or thin 3. Density profile of the circumnuclear regions can play a role: cusp or core etc… etc… Blois 2008

A sample of Low Luminosity AGN II. LOW LUMINOSITY AGN DO THEY HAVE JETS? YES! A sample of Low Luminosity AGN large M(BH) small M(BH) (bulge) Falcke et al; 2000 Compact jet structure with flat spectra observed in 40% of LLAGN Blois 2008 but no detailed mechanism proposed so far

FINALLY IS THE SOLUTION THIS ONE? Radio Quiet AGN Radio Loud AGN Blois 2008

OR ARE THE WIND AND THE JET COEXISTING? Hawley, Balbus, 2002 inner jets can be undetected in luminous AGN Blois 2008

AND FINALLY, VERY LITTLE IS YET UNDERSTOOD! CONCLUSION 1. jets or high energy mechanisms can escape detection, if they are quenched close to the BH 2. Jets in radio loud high luminosity AGN are likely driven by spinning black holes, but other mechanisms must play a role 3. BAD NEWS: Only a small proportion of luminous AGN have relativistic jets and non-thermal radiation 4. GOOD NEWS: In low luminosity AGN (and basically all galaxies), jets and high energy processes take place close to the central BH AND FINALLY, VERY LITTLE IS YET UNDERSTOOD! Blois 2008

Blois 2008

An exemple of a strong accretor (Ton S 180) modeled by a thick disk, M(BH)=6 106 Mo, m=60 Blois 2008 Kawaguchi, Piérens, Huré, 2003

Caution: one defines sometimes Blois 2008

Wind driving mechanism radiation pressure driven from the disk but « shielding » of the central source necessary centrifugally driven from disks threated by an open magnetic field - thermally or hydrodynamically driven from the hot corona sketch of a disk wind, centrifugally and/or radiatively accelerated Blois 2008